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arXiv · 1605.02369

The $m=1$ instability \& gravitational wave signal in binary neutron star mergers

Luis Lehner·Steven L. Liebling·Carlos Palenzuela·Patrick Motl
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Abstract

We examine the development and detectability of the $m=1$ instability in the remnant of binary neutron star mergers. The detection of the gravitational mode associated with the $m=1$ degree of freedom could potentially reveal details of the equation of state. We analyze the post-merger epoch of simulations of both equal and non-equal mass neutron star mergers using three realistic, microphysical equations of state and neutrino cooling. Our studies show such an instability develops generically and within a short dynamical time to strengths that are comparable or stronger than the $m=2$ mode which is the strongest during the early post-merger stage. We estimate the signal to noise ratio that might be obtained for the $m=1$ mode and discuss the prospects for observing this signal with available Earth-based detectors. Because the $m=1$ occurs at roughly half the frequency of the more powerful $m=2$ signal and because it can potentially be long-lived, targeted searches could be devised to observe it. We estimate that with constant amplitude direct detection of the mode could occur up to a distance of roughly $14\,\mathrm{Mpc}$ whereas a search triggered by the inspiral signal could extend this distance to roughly $100\,\mathrm{Mpc}$.

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Luis Lehner, Steven L. Liebling, Carlos Palenzuela, Patrick Motl. 2016-05-08. The $m=1$ instability \& gravitational wave signal in binary neutron star mergers. https://doi.org/10.1103/physrevd.94.043003

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